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SZ Crateris is a binary star system in the southern constellation Crater. Both components belong to the main sequence: the primary star has a spectral classification of K5V while the secondary is a red dwarf of spectral class M0V. The radius of the primary is about 66% the radius of the Sun, while the secondary member is only about 42% of the solar radius. In 1994, the two stars were separated by 5.1 arc seconds, which is equivalent to 112.41 astronomical units.[7]

SZ Crateris

A visual band light curve for SZ Crateris, adapted from Cutispoto et al. (2001)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Crater
Right ascension 11h 21m 26.6645s[2]
Declination −20° 27′ 13.619″[2]
Apparent magnitude (V) 8.61/11.0[3]
Characteristics
Spectral type K7V/M2.5Ve[4]
U−B color index +1.20[5]
B−V color index +1.36[5]
Variable type BY Dra
Astrometry
A
Radial velocity (Rv)−0.11[6] km/s
Proper motion (μ) RA: +181.231[6] mas/yr
Dec.: −92.306[6] mas/yr
Parallax (π)76.4165 ± 0.0821 mas[6]
Distance42.68 ± 0.05 ly
(13.09 ± 0.01 pc)
Absolute magnitude (MV)+7.75[7]
B
Radial velocity (Rv)−2.86[8] km/s
Proper motion (μ) RA: +220.306[8] mas/yr
Dec.: −129.404[8] mas/yr
Parallax (π)76.3549 ± 0.0955 mas[8]
Distance42.72 ± 0.05 ly
(13.10 ± 0.02 pc)
Absolute magnitude (MV)+10.0[7]
Orbit[9]
Period (P)714.6 yr
Semi-major axis (a)5.896″
Eccentricity (e)0.63
Details
A
Radius0.63[6] R☉
Luminosity0.109[6] L☉
Surface gravity (log g)4.5[10] cgs
Temperature4,162[6] K
Metallicity [Fe/H]0.04[10] dex
Rotational velocity (v sin i)4.5[10] km/s
B
Radius0.42[11] R☉
Luminosity0.06[12] L☉
Temperature3,670[12] K
Age194±20[13] Myr
Other designations
SZ Crt, BD-19 3242, GJ 425, HD 98712, SAO 179801, HIP 55454
A: LTT 4204[14]
B: LTT 4205[15]
Database references
SIMBADdata
A
B

SZ Crateris is classified as a marginal BY Draconis variable, and has an optical variability cycle of 11.58 days. (The star causing the variability is unspecified.)[16] Compared to the Sun, SZ Crateris has a slightly higher proportion of elements other than hydrogen and helium.[10] Based upon gyrochronology, the estimated age of this star is under 200 million years.[13]

The SZ Crateris system is a member of the Ursa Major moving group of stars that have similar motions through space.[10] The space velocity components of this system are U = +13.86 ± 0.37, V = –3.51 ± 1.97 and W = +1.65 ± 1.53 km/s.[17] It is on an orbit through the Milky Way that has an orbital eccentricity of 0.092, which will bring it as close as 26.06 kly (7.99 kpc) to the galactic core, and as distant as 31.31 kly (9.60 kpc). The inclination of the orbit carries the system as much as 0.352 kly (0.108 kpc) from the plane of the galactic disk.[18]


References


  1. Cutispoto, G.; Messina, S.; Rodono, M. (March 2001). "Long-term monitoring of active stars IX. Photometry collected in 1993". Astronomy & Astrophysics. 367: 910–930. doi:10.1051/0004-6361:20000549. Retrieved 17 December 2021.
  2. Perryman, M. A. C.; Lindegren, L.; Kovalevsky, J.; Hog, E.; Bastian, U.; Bernacca, P. L.; Creze, M.; Donati, F.; Grenon, M.; Grewing, M.; Van Leeuwen, F.; Van Der Marel, H.; Mignard, F.; Murray, C. A.; Le Poole, R. S.; Schrijver, H.; Turon, C.; Arenou, F.; Froeschle, M.; Petersen, C. S. (1997). "The HIPPARCOS Catalogue". Astronomy & Astrophysics. 323: 501. Bibcode:1997A&A...323L..49P.
  3. Reid, I. Neill; Cruz, Kelle L.; Allen, Peter R.; Mungall, Finlay; Kilkenny, David; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2004). "Meeting the Cool Neighbors. VIII. A Preliminary 20 Parsec Census from the NLTT Catalogue". The Astronomical Journal (Submitted manuscript). 128 (1): 463. arXiv:astro-ph/0404061. Bibcode:2004AJ....128..463R. doi:10.1086/421374. S2CID 28314795.
  4. Alonso-Floriano, F. J.; Morales, J. C.; Caballero, J. A.; Montes, D.; Klutsch, A.; Mundt, R.; Cortés-Contreras, M.; Ribas, I.; Reiners, Ansgar; Amado, P. J.; Quirrenbach, A.; Jeffers, S. V. (2015). "CARMENES input catalogue of M dwarfs" (PDF). Astronomy & Astrophysics. 577: A128. arXiv:1502.07580. doi:10.1051/0004-6361/201525803. S2CID 53135130.
  5. Corben, P. M.; Carter, B. S.; Banfield, R. M.; Harvey, G. M. (1972). "U, B, V photometry of 500 southern stars". Monthly Notes of the Astronomical Society of South Africa. 31: 7–22. Bibcode:1972MNSSA..31....8C.
  6. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  7. Poveda, A.; Herrera, M. A.; Allen, C.; Cordero, G.; Lavalley, C. (1994). "Statistical studies of visual double and multiple stars. II. A catalogue of nearby wide binary and multiple systems". Revista Mexicana de Astronomía y Astrofísica. 28: 43. Bibcode:1994RMxAA..28...43P.
  8. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  9. Malkov, O. Yu.; Tamazian, V. S.; Docobo, J. A.; Chulkov, D. A. (2012). "Dynamical masses of a selected sample of orbital binaries". Astronomy and Astrophysics. 546: A69. Bibcode:2012A&A...546A..69M. doi:10.1051/0004-6361/201219774.
  10. Paulson, Diane B.; Yelda, Sylvana; Allen, Peter R.; Kilkenny, David; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2006). "Differential Radial Velocities and Stellar Parameters of Nearby Young Stars". The Publications of the Astronomical Society of the Pacific. 118 (843): 706–715. arXiv:astro-ph/0605433. Bibcode:2006PASP..118..706P. doi:10.1086/504115. S2CID 16194615.
  11. Johnson, H. M.; Wright, C. D. (1983). "Predicted infrared brightness of stars within 25 parsecs of the sun". The Astrophysical Journal Supplement Series. 53: 643. Bibcode:1983ApJS...53..643J. doi:10.1086/190905.
  12. Morales, J. C.; Ribas, I.; Jordi, C.; Kilkenny, David; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2008). "The effect of activity on stellar temperatures and radii". Astronomy and Astrophysics. 478 (2): 507. arXiv:0711.3523. Bibcode:2008A&A...478..507M. doi:10.1051/0004-6361:20078324. S2CID 16238033.
  13. Barnes, Sydney A. (2007). "Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors". The Astrophysical Journal. 669 (2): 1167–1189. arXiv:0704.3068. Bibcode:2007ApJ...669.1167B. doi:10.1086/519295. S2CID 14614725.
  14. "V* SZ Crt -- Variable of BY Dra type". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-02-18.
  15. "LTT 4205 -- High proper-motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-02-18.
  16. Cutispoto, G. (1996). "Long-term monitoring of active stars. V. UBV(RI)_ c_ photometry collected in Feb.-Mar. 1990". Astronomy and Astrophysics Supplement. 119 (2): 281–292. Bibcode:1996A&AS..119..281C. doi:10.1051/aas:1996245.
  17. Karataș, Yüksel; Bilir, ‪Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2004). "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution". Monthly Notices of the Royal Astronomical Society. 349 (3): 1069–1092. arXiv:astro-ph/0404219. Bibcode:2004MNRAS.349.1069K. doi:10.1111/j.1365-2966.2004.07588.x. S2CID 15290475.
  18. Allen, C.; Herrera, M. A. (1998). "The Galactic Orbits of Nearby UV Ceti Stars". Revista Mexicana de Astronomía y Astrofísica. 34: 37. Bibcode:1998RMxAA..34...37A.

На других языках

- [en] SZ Crateris

[ru] SZ Чаши

SZ Чаши (SZ Crateris, сокращ. SZ Crt) — двойная звезда в южном созвездии Чаши. SZ Чаши состоит из двух звёзд, имеющих видимую звёздную величину +8,61m[13] и 11.0m[13], и, согласно шкале Бортля, они обе не видны невооружённым глазом.


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